Relativistic jets associated with active galactic nuclei (AGN) produce radiation over a large range of the electromagnetic spectrum. While relativistic magneto-hydrodynamic (RMHD) simulations have become a powerful tool to model the physical structure of jets, in order to correlate them to observations, estimates of the radiation must also be determined. We present the initial results from a study to calculate the multi-wavelength radiation by applying Monte-Carlo methods, using the parameters provided by the RMHD simulations. We present our initial implementation of a Monte Carlo code that interfaces with the RMHD simulation of a steady state axis-symmetric jet created using the PLUTO code. Properties such as the number density, energy density, magnetic field and bulk Lorentz factor are obtained from the RMHD simulations and used to generate a synchrotron photon distribution in each cell. These photons are tracked as they move through the simulation environment and undergoes inverse Compton scattering. Each photon is recorded when it exits the simulation domain and is used to construct multi-wavelength SEDs and light curves. This will provide a time-dependent, multi-zone Synchrotron Self-Compton (SSC) emission model for RMHD simulations.